Testing the turbulent origin of the stellar initial mass function
نویسندگان
چکیده
Supersonic turbulence in the interstellar medium (ISM) is closely linked to formation of stars, and hence many theories connect stellar initial mass function (IMF) with turbulent properties molecular clouds. Here we test three turbulence-based IMF models (by Padoan & Nordlund 2002, Hennebelle Chabrier 2008, Hopkins 2012), which predict relation between high-mass slope ($\Gamma$) IMF, $\mathrm{d} N/\mathrm{d} \log M \propto M^{\Gamma}$ exponent n velocity power spectrum turbulence, $E_v(k)\propto k^{-n} $, where $n\approx 2$ corresponds typical ISM turbulence. Using hydrodynamic simulations, drive an unusual index 1$, measure $\Gamma$, compare results 2$. We find that reducing $n$ from 2 1 primarily changes region (beyond median mass), slopes within 95 per cent confidence interval $-1.5<\Gamma<-1$ for $n \approx 1$ $-3.7<\Gamma<-2.4$ 2$, respectively. Thus, $n=1$ a significantly flatter more massive stars formed than these simulations predictions theories. while theory matches our fair accuracy, other either fail reproduce main qualitative outcome or require some modifications. conclude plays key role shaping shallower producing stars.
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ژورنال
عنوان ژورنال: Monthly Notices of the Royal Astronomical Society
سال: 2021
ISSN: ['0035-8711', '1365-8711', '1365-2966']
DOI: https://doi.org/10.1093/mnras/stab505